(a) Frequency distribution of 3 mm continuum fluxes measured toward the low‐mass NGC 2024 K‐band cluster members within the unit gain contour of the OVRO mosaic (histogram). IRS 2 is off the scale of the plot at ~0.1 Jy. The three sources with fluxes 2.5 mJy correspond to slight offsets from FIR 2 and FIR 4 (§ 4) and to part of the NCP structure. The extremely negative source with ﹩F\sim -4﹩ mJy is actually tracing a sidelobe artifact. (b) Frequency distribution of 3 mm continuum fluxes for all pixels within the unit gain contour of the high angular resolution OVRO map (Fig. 5), where the bright (>3.75 mJy) point sources listed in Table 1 have been removed using CLEAN (histogram). In both panels, the frequency distribution expected for Gaussian noise with a mean of 0 and an rms of 0.75 mJy is indicated by a dotted line.