  We analyzed the light curves of 1376 early-to-late, nearby M dwarfs to search
for white-light flares using photometry from the All-Sky Automated Survey for
Supernovae (ASAS-SN). We identified 480 M dwarfs with at least one potential
flare employing a simple statistical algorithm that searches for sudden
increases in $V$-band flux. After more detailed evaluation, we identified 62
individual flares on 62 stars. The event amplitudes range from $0.12 <\Delta V
< 2.04$ mag. Using classical-flare models, we place lower limits on the flare
energies and obtain $V$-band energies spanning $2.0\times10^{30} \lesssim E_{V}
\lesssim 6.9\times10^{35}$ erg. The fraction of flaring stars increases with
spectral type, and most flaring stars show moderate to strong H$\alpha$
emission. Additionally, we find that 14 of the 62 flaring stars are rotational
variables, and they have shorter rotation periods and stronger H$\alpha$
emission than non-flaring rotational variable M dwarfs.
