  We present analyses of near-infrared, spectroscopic data from the Apache
Point Observatory Galactic Evolution Experiment (APOGEE) survey for 45
previously confirmed or candidate white dwarf-main sequence (WDMS) binaries
identified by the optical SDSS and LAMOST surveys. Among these 45 systems, we
classify three as having red giant primaries in the LAMOST sample and fourteen
to be young stellar object contaminants in the photometrically identified SDSS
sample. From among the subsample of 28 systems that we confirm to have MS
primaries, we derive and place limits on orbital periods and velocity
amplitudes for fourteen. Seven systems have significant velocity variations
that warrant a post-common-envelope (PCE) binary classification -- four of
which are newly classified, three of which are newly confirmed, and five for
which we can derive full orbital parameters. If confirmed, one of these newly
discovered systems (2M14544500+4626456) will have the second longest orbital
period reported for a typical, compact PCE WDMS binary ($P=15.1$ days). In
addition to the seven above, we also recover and characterize with APOGEE data
the well known PCE WDMS systems EG UMa and HZ 9. We also investigate the
overall metallicity distribution of the WDMS sample, which is a parameter space
not often explored for these systems. Of note, we find one system
(2M14244053+4929580) to be extremely metal-poor (${\rm [Fe/H]}=-1.42$) relative
to the rest of the near-solar sample. Additionally, the PCE systems in our
sample are found to be, on average, higher in metallicity than their
wide-binary counterparts, though we caution that with this small number of
systems, the sample may not be representative of the overall distribution of
WDMS systems.
