  The physical parameters of the retired A star HD 185351 were analysed in
great detail by Johnson et al. (2014) using interferometry, spectroscopy and
asteroseismology. Results from all independent methods are consistent with HD
185351 having a mass in excess of $1.5\mathrm{M}_{\odot}$. However, the study
also showed that not all observational constraints could be reconciled in
stellar evolutionary models, leading to mass estimates ranging from $\sim
1.6-1.9\mathrm{M}_{\odot}$ and casting doubts on the accuracy of stellar
properties determined from asteroseismology. Here we solve this discrepancy and
construct a theoretical model in agreement with all observational constraints
on the physical parameters of HD 185351. The effects of varying input physics
are examined as well as considering the additional constraint of the observed
g-mode period spacing. This quantity is found to be sensitive to the inclusion
of additional mixing from the convective core during the main sequence, and can
be used to calibrate the overshooting efficiency using low-luminosity red giant
stars. A theoretical model with metallicity
$\left[\mathrm{Fe/H}\right]=0.16$dex, mixing-length parameter
$\alpha_{\mathrm{MLT}}=2.00$, and convective overshooting efficiency parameter
$f=0.030$ is found to be in complete agreement with all observational
constraints for a stellar mass of $M\simeq1.60\mathrm{M}_{\odot}$.
