  We present a suite of seven 3D supernova simulations of non-rotating low-mass
progenitors using multi-group neutrino transport. Our simulations cover single
star progenitors with zero-age main sequence masses between $9.6 M_\odot$ and
$12.5 M_\odot$ and (ultra)stripped-envelope progenitors with initial helium
core masses between $2.8 M_\odot$ and $3.5 M_\odot$. We find explosion energies
between $0.1\,\mathrm{Bethe}$ and $0.4\,\mathrm{Bethe}$, which are still rising
by the end of the simulations. Although less energetic than typical events, our
models are compatible with observations of less energetic explosions of
low-mass progenitors. In six of our models, the mass outflow rate already
exceeds the accretion rate onto the proto-neutron star, and the mass and
angular momentum of the compact remnant have closely approached their final
value, barring the possibility of later fallback. While the proto-neutron star
is still accelerated by the gravitational tug of the asymmetric ejecta, the
acceleration can be extrapolated to obtain estimates for the final kick
velocity. We obtain gravitational neutron star masses between $1.22 M_\odot$
and $1.44 M_\odot$, kick velocities between $11\, \mathrm{km}\,
\mathrm{s}^{-1}$ and $695\, \mathrm{km}\, \mathrm{s}^{-1}$, and spin periods
from $20\, \mathrm{ms}$ to $2.7\,\mathrm{s}$, which suggests that typical
neutron star birth properties can be naturally obtained in the neutrino-driven
paradigm. We find a loose correlation between the explosion energy and the kick
velocity. There is no indication of spin-kick alignment, but a correlation
between the kick velocity and the neutron star angular momentum, which needs to
be investigated further as a potential point of tension between models and
observations.

Solar and Stellar Astrophysics;High Energy Astrophysical Phenomena