  We present a study of the relationship between galactic kinematics, flare
rates, chromospheric activity, and rotation periods for a volume-complete,
nearly all-sky sample of 219 single stars within 15 parsecs and with masses
between 0.1$-$0.3 M$_{odot}l$ observed during the primary mission of TESS. We
find all stars are consistent with a common value of $\alpha$=1.984 $\pm$ 0.019
for the exponent of the flare frequency distribution. Using our measured
stellar radial velocities and Gaia astrometry, we determine galactic UVW space
motions. We find 64% of stars are members of the Galactic thin disk, 5% belong
to the thick disk, and for the remaining 31%, we cannot confidently assign
membership to either component. If we assume star formation has been constant
in the thin disk for the past 8 Gyr, then based on the fraction that we observe
to be active, we estimate the average age at which these stars transition from
the saturated to the unsaturated flaring regime to be 2.4 $\pm$ 0.3 Gyr. This
is consistent with the ages that we assign from galactic kinematics: We find
that stars with Prot $<$ 10 days have an age of 2.0 $\pm$ 1.2 Gyr, stars with
10 $<$ Prot $\leq$ 90 days have an age of 5.6 $\pm$ 2.7 Gyr, and stars with
Prot $>$ 90 days have an age of 12.9 $\pm$ 3.5 Gyr. We find that the average
age of stars with Prot $<$ 10 days increases with decreasing stellar mass from
0.6 $\pm$ 0.3 Gyr (0.2 - 0.3 M$_{odot}$) to 2.3 $\pm$ 1.3 Gyr (0.1--0.2
M$_{odot}l$).
