  APOGEE spectra offer $\lesssim$1 km s$^{-1}$ precision in the measurement of
stellar radial velocities (RVs). This holds even when multiple stars are
captured in the same spectrum, as happens most commonly with double-lined
spectroscopic binaries (SB2s), although random line of sight alignments of
unrelated stars can also occur. We develop a code that autonomously identifies
SB2s and higher order multiples in the APOGEE spectra, resulting in 7273
candidate SB2s, 813 SB3s, and 19 SB4s. We estimate the mass ratios of binaries,
and for a subset of these systems with sufficient number of measurements we
perform a complete orbital fit, confirming that most systems with period $<$10
days have circularized. Overall, we find a SB2 fraction ($F_{SB2}$) $\sim$3\%
among main sequence dwarfs, and that there is not a significant trend in
$F_{SB2}$ with temperature of a star. We are also able to recover a higher
$F_{SB2}$ in sources with lower metallicity, however there are some
observational biases. We also examine light curves from TESS to determine which
of these spectroscopic binaries are also eclipsing. Such systems, particularly
those that are also pre- and post-main sequence, are good candidates for a
follow-up analysis to determine their masses and temperatures.
