  The Hyades, Praesepe, and Pleiades are well studied stellar clusters that
anchor important secondary stellar age indicators. Recent studies have shown
that main sequence turn off-based ages for these clusters may depend on the
degree of rotation in the underlying stellar models. Rotation induces
structural instabilities that can enhance the chemical mixing of a star,
extending its fuel supply. In addition, rotation introduces a modulation of the
star's observed magnitude and color due to the effects of gravity darkening. We
aim to investigate the extent to which stellar rotation affects the age
determination of star clusters. We utilize the MESA stellar evolution code to
create models that cover a range of rotation rates corresponding to
$\Omega/\Omega_c=0.0$ to $0.6$ in $0.1$ dex steps, allowing the assessment of
variations in this dimension. The statistical analysis package, MATCH, is
employed to derive ages and metallicities by fitting our MESA models to Tycho
$B_T$, $V_T$ and 2MASS $J$, $K_s$ color-magnitude diagrams. We find that the
derived ages are relatively insensitive to the effects of rotation. For the
Hyades, Praesepe, and Pleiades, we derive ages based on synthetic populations
that model a distribution of rotation rates or a fixed rate. Across each case,
derived ages tend to agree roughly within errors, near $680$, $590$, and
$110-160$ Myr for the Hyades, Praesepe, and Pleiades, respectively. These ages
are in agreement with Li depletion boundary-based ages and previous analyses
that used non-rotating isochrones. Our methods do not provide a strong
constraint on the metallicities of these clusters.
