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APOGEE spectra offer $\lesssim$1 km s$^{-1}$ precision in the measurement ofstellar radial velocities (RVs). This holds even when multiple stars arecaptured in the same spectrum, as happens most commonly with double-linedspectroscopic binaries (SB2s), although random line of sight alignments ofunrelated stars can also occur. We develop a code that autonomously identifiesSB2s and higher order multiples in the APOGEE spectra, resulting in 7273candidate 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 weperform a complete orbital fit, confirming that most systems with period $<$10days have circularized. Overall, we find a SB2 fraction ($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 someobservational biases. We also examine light curves from TESS to determine whichof these spectroscopic binaries are also eclipsing. Such systems, particularlythose that are also pre- and post-main sequence, are good candidates for afollow-up analysis to determine their masses and temperatures.

Double-lined spectroscopic binaries in the APOGEE DR16 and DR17 data