  We present analysis of nearly 1,000 near-infrared, integrated light spectra
from APOGEE in the inner $\sim$7 kpc of M31. We utilize full spectrum fitting
with A-LIST simple stellar population spectral templates that represent a
population of stars with the same age, [M/H], and [$\alpha$/M]. With this, we
determine the mean kinematics, metallicities, $\alpha$ abundances, and ages of
the stellar populations of M31's bar, bulge, and inner disk ($\sim$4-7 kpc). We
find a non-axisymmetric velocity field in M31 resulting from the presence of a
bar. The bulge of M31 is metal-poor relative to the disk ([M/H] =
$-0.149^{+0.067}_{-0.081}$ dex), features minima in metallicity on either side
of the bar ([M/H] $\sim$ -0.2), and is enhanced in $\alpha$ abundance
([$\alpha$/M] = $0.281^{+0.035}_{-0.038}$). The disk of M31 within $\sim$7 kpc
is enhanced in both metallicity ([M/H] = $-0.023^{+0.050}_{-0.052}$) and
$\alpha$ abundance ([$\alpha$/M] = $0.274^{+0.020}_{-0.025}$). Both of these
structural components are uniformly old at $\simeq$ 12 Gyr. We find the
metallicity increases with distance from the center of M31, with the steepest
gradient along the disk major axis ($0.043\pm0.021$ dex/kpc). This gradient is
the result of changing light contributions from the metal-poor bulge and
metal-rich disk. The chemodynamics of stellar populations encodes information
about a galaxy's chemical enrichment, star formation history, and merger
history, allowing us to discuss new constraints on M31's formation. Our results
provide a stepping stone between our understanding of the Milky Way and other
external galaxies.
