Projected separation distributions for various populations of M-dwarf multiples. The histogram shows the distribution of projected separations for the targets in the 15 pc POKEMON sample that are known to be multiple, separated by planet-hosting (orange) and non–planet-hosting (white) status. The dotted, black line is a Gaussian fit to the projected separations of the non–planet-hosting POKEMON multiples, with a peak at 5.57 au (﹩{\sigma }_{\mathrm{log}a}=1.3﹩, ﹩{\mathrm{SE}}_{\mathrm{log}a}=0.11﹩). The dashed, orange line is a Gaussian fit to the projected separations of the planet-hosting POKEMON multiples, with a peak at 198 au (﹩{\sigma }_{\mathrm{log}a}=0.77﹩, ﹩{\mathrm{SE}}_{\mathrm{log}a}=0.32﹩). The solid, yellow line is a Gaussian fit to the projected separations of the M-dwarf TOIs from Clark et al. (2022a), with a peak at 735 au (﹩{\sigma }_{\mathrm{log}a}=0.83﹩, ﹩{\mathrm{SE}}_{\mathrm{log}a}=0.25﹩). We note that we use Gaussian fits to compare our distribution of projected separations with other studies of multiplicity (e.g., Raghavan et al. 2010; Winters et al. 2019a); we do not use this to indicate that the distribution of stellar multiples is Gaussian, but rather to show that the peaks of the distributions are shifted. The two planet-hosting distributions have peaks at relatively consistent values, whereas the peaks of the planet-hosting and non–planet-hosting distributions differ by more than an order of magnitude. This result indicates that the presence of a stellar companion impacts the formation and long-term stability of any planets in the system.