  Stellar ages are critical for understanding the temporal evolution of a
galaxy. We calculate the ages of over 6000 red giant branch stars in the Large
Magellanic Cloud (LMC) observed with SDSS-IV / APOGEE-S. Ages are derived using
multi-band photometry, spectroscopic parameters (T$_\text{eff}$, $\log{g}$,
[Fe/H], and [$\alpha$/Fe]) and stellar isochrones and the assumption that the
stars lie in a thin inclined plane to get accurate distances. The isochrone age
and extinction are varied until a best match is found for the observed
photometry. We perform validation using the APOKASC sample, which has
asteroseismic masses and accurate ages, and find that our uncertainties are
$\sim$20% and range from $\sim$1$-$3 Gyr for the calculated age values. Here we
present the LMC age map as well as the age-radius relation and an accurate
age-metallicity relation (AMR). The age map and age-radius relation reveal that
recent star formation in the galaxy was more centrally located and that there
is a slight dichotomy between the north and south with the northern fields
being slightly younger. The northern fields that cover a known spiral arm have
median ages of $\gtrsim$ 2 Gyr, which is the time when an interaction with the
SMC is suggested to have happened. The AMR is mostly flat especially for older
ages although recently (about 2.0-2.5 Gyr ago) there is an increase in the
median [Fe/H]. Based on the time frame, this might also be attributed to the
close interaction between the LMC and SMC.

Astrophysics of Galaxies