  Using modern isochrones with customized physics and carefully considered
statistical techniques, we recompute the age distribution for a sample of 91
micro-lensed dwarfs in the Galactic bulge presented by Bensby et al. (2017) and
do not produce an age distribution consistent with their results. In
particular, our analysis finds that only 15 of 91 stars have ages younger than
7 Gyr, compared to their finding of 42 young stars in the same sample. While we
do not find a constituency of very young stars, our results do suggest the
presence of an $\sim8$ Gyr population at the highest metallicities, thus
contributing to long-standing debate about the age--metallicity distribution of
the Galactic bulge. We supplement this with attempts at independent age
determinations from two sources of photometry, BDBS and \textit{Gaia}, but find
that the imprecision of photometric measurements prevents reliable age and age
uncertainty determinations. Lastly, we present age uncertainties derived using
a first-order consideration of global modeling uncertainties in addition to
standard observational uncertainties. The theoretical uncertainties are based
on the known variance of free parameters in the 1D stellar evolution models
used to generate isochrones, and when included, result in age uncertainties of
$2$--$5$ Gyr for this spectroscopically well-constrained sample. These error
bars, which are roughly twice as large as typical literature values, constitute
realistic lower limits on the true age uncertainties.
