The scenario you have proposed has more problems than just the L3 point's instability. You also have issues with mass, interaction with other planet's gravity, and the shape of Earth's orbit.
Starting with the mass problem: In order for a Counter-earth to exist, it must have precisely the same mass as Earth does. This is because orbital equations mandate that orbital velocity is a factor of mass and distance from the gravitational body. Assuming a circular orbit to simplify things...
$$ v = \sqrt{\frac{GM}{r}} $$
If you wish to maintain velocity with a smaller mass, you must move it closer to the body it is orbiting. The L3 point has forces that try to hold you at a similar orbital velocity, but they wouldn't be strong enough to hold an entire planet there. If your planet had a lower mass, and thus higher velocity than Earth, then it is going to have a wildly elliptical orbit with a different orbital period (meaning we'd have probably crashed into each other by now if we are in the same plane)
Orbital shape is also an issue. Since Earth sits in an elliptical orbit, in order to sit constantly in Earth's L3, Counter-Earth would need a matching elliptical orbit that is precisely the opposite of Earth's. Your energy needs for station keeping would vary depending on the time of year.
For a lower mass planet, with Earth's same orbital velocity, your challenge would be keeping the planet from sliding further out on Earth's orbital path because of its lower mass.
Now, on to the Lagrange Point issue. The L3 point is the spot at which Earth and the Sun's gravitational pulls line up, so there is no angular force tugging you off-station. Beyond that, it is your centrifugal force from orbital velocity that holds you on-station with respect to distance from the sun. 801
With a mass smaller than the Earth, you would tend to drift further from the sun, so station keeping would mandate that you exert an force propelling you inward towards the sun. Further complications will be introduced by the orbits of other planets, particularly Venus, which will tug inwards.
Now...on to the math. Ignoring Venus for a moment, lets calculate the gravitational force generated by the Earth/Sun system that you are in the L3 point of. Note that I am also ignoring the in/out drift of Earth and Counter-Earth for this in the name of simplicity and am using the Average distance. If you want to calculate minimum and maximum energy requirements, swap out the distances for the Earth's aphelion distance and perihelion distance. (Remember to double the distance for the gravitational pull between Earth and Counter-Earth)
Force of Gravity can be calculated like so...
$$ Fg = \frac{Gm1m2}{r^2} $$
So, to get total Force of Gravity for the system...
$$ F = \frac{Gm1.989e^{30}}{149,597,870,700^2} + \frac{Gm5.972e^{24}}{299,195,741,400^2} $$
Where m is the mass of your planet and G is the Gravitational Constant $6.6726e^{-11}$
Plugging in the '85% Earth Mass' value that you gave, we get a Force of Gravity equal to $3.0119e^{22}N$. In order for our planet to neither fly away, nor fall into the sun, we need for its Centrifugal force (+ generated force) to be equal to the force of Gravity.
So, calculating the natural Centrifugal force of our planet, moving at Earth's orbital velocity renders this equation:
$$ F = \frac{mv^2}{r} $$
For the sake of simplicity, we are going to ignore the fact that the orbital center is not the center of the sun...it's a little bit off, but not by much. So, plugging in values gives us this finalized equation...
$$ F = \frac{m*30,000^2}{149597870700} $$
Again plugging in our 85% mass, we get a Centrifugal force of: $3.0539e^{22}N$
This leaves us having to make up for $4.2015e^{20}N$ of Force on a constant basis. These forces give the planet an outward acceleration of $.0000828m/s^2$ (using $a=\frac{F}{m}$). Calculating for displacement using...
$$ x = vt+.5at^2 $$
Shows that our planet will attempt to slip off station by $.0000414m$ every second. This is a quite small number, but we have to keep it perfectly balanced. 24