  The relationship between age, rotation, and magnetic activity can be used to
roughly estimate the ages of solar-type stars. At lower stellar masses, the
relationship between activity and age changes due to the less efficient angular
momentum loss, and may disappear entirely for ultracool (late-M and L) dwarfs.
The detection of flares (as a tracer of magnetic activity) can be combined with
kinematic tracers of age to explore the relationship between age and activity
for ultracool dwarfs. The final data release of GAIA will provide time-resolved
photometry of GAIA targets in the $G$ filter, but the effect of flares in the
$G$-band is not well understood. I use a simple flare model to estimate the
conversion of flare magnitudes for M3--L5 dwarfs in the Johnson $V$-, SDSS
$r$-, and Kepler- bands to the GAIA $G$-band. By applying those conversions to
previously observed flare rates, I estimate that M0-M6 dwarfs will have a flare
rate in GAIA of $R_{f,GAIA} \gtrsim 8.73 \times 10^{-4}~{\rm hr}^{-1}~{\rm
deg}^{-2}$, corresponding to a total of $\gtrsim$20,000 flares in the whole
survey. If ultracool dwarfs have the same flare rate, I would expect a total of
$\gtrsim$20 flares on M7-L5 dwarfs.
