  We present $BVI$ surface photometry of 31 dwarf galaxy candidates discovered
in a deep image stack from the KMTNet Supernova Program of $\sim$ 30 square
degrees centered on the nearby NGC 2784 galaxy group. Our final images have a
3$\sigma$ surface brightness detection limit of $\mu_V\approx 28.5$ mag
arcsec$^{-2}$. The faintest central surface brightness that we measure is
$\mu_{0,V} = 26.1$ mag arcsec$^{-2}$. If these candidates are at the distance
of NGC 2784, then they have absolute magnitudes greater than $M_V = -9.5$ mag
and effective radii larger than 170 pc. Their radial number density decreases
exponentially with distance from the center of NGC 2784 until it flattens
beyond a radius of 0.5 Mpc. We interpret the baseline density level to
represent the background contamination and so estimate that 22 of the 31 new
candidates are dwarf members of the group. The candidate's average color,
$\langle (B-V)_0\rangle\approx 0.7$, and Sersic structural parameters are
consistent with those parameters for the dwarf populations of other groups. We
find that the central population of dwarfs is redder and brighter than the rest
of the population. The measured faint end slope of the luminosity function,
$\alpha\approx-1.33$, is steeper than that of the Local Group but consistent
with published results for other groups. Such comparisons are complicated by
systematic differences among different studies, but will be simpler when the
KMTNet survey, which will provide homogenous data for 15 to 20 groups, is
completed.
