Determining the magnitude and rate at which low mass stars flare is an important problem in stellar astrophysics because flares are a major source of variability in large time domain surveys, affect the atmospheres of orbiting planetary systems, and are manifestations of magnetic field production and reconfiguration, processes which are not well understood on M dwarfs. We present early results from a multi-year observing campaign to statistically determine M dwarf flare rates and energies as a function of spectral type and activity level. Our observations consist of over 100 hours of monitoring M dwarfs on three telescopes. In addition to preliminary flare rates, we discuss our method of determining energy and duration.