  Stars are known to be more active when they are young, resulting in a strong
correlation between age and photometric variability. The amplitude variation
between stars of a given age is large, but the age-variability relation becomes
strong over large groups of stars. We explore this relation using the excess
photometric uncertainty in Gaia photometry ($Var_{G}$, $Var_{BP}$, and
$Var_{RP}$) as a proxy for variability. The metrics follow a Skumanich-like
relation, scaling as $\simeq t^{-0.4}$. By calibrating against a set of
associations with known ages, we show how $Var$ of population members can
predict group ages within 10-20% for associations younger than $\simeq$2.5 Gyr.
In practice, age uncertainties are larger, primarily due to finite group size.
The index is most useful at the youngest ages ($<$100 Myr), where the
uncertainties are comparable to or better than those derived from a
color-magnitude diagram. The index is also widely available, easy to calculate,
and can be used at intermediate ages where there are few or no pre- or
post-main-sequence stars. We further show how $Var$ can be used to find new
associations and test if a group of co-moving stars is a real co-eval
population. We apply our methods on the Theia groups within 350 pc and find
$\gtrsim$90% are inconsistent with drawing stars from the field and $\simeq$80%
have variability ages consistent with those derived from the CMD. Our finding
suggest the great majority of these groups contain real populations.
