  The \textit{absolute age} of a simple stellar population is of fundamental
interest for a wide range of applications but is difficult to measure in
practice, as it requires an understanding of the uncertainties in a variety of
stellar evolution processes as well as the uncertainty in the distance,
reddening and composition. As a result, most studies focus only on the
\textit{relative age} by assuming that stellar evolution calculations are
accurate and using age determinations techniques that are relatively
independent of distance and reddening. Here, we construct $20,000$ sets of
theoretical isochrones through Monte Carlo simulation using the Dartmouth
Stellar Evolution Program to measure the absolute age of the globular cluster
M92. For each model, we vary a range of input physics used in the stellar
evolution models, including opacities, nuclear reaction rates, diffusion
coefficients, atmospheric boundary conditions, helium abundance, and treatment
of convection. We also explore variations in the distance and reddening as well
as its overall metallicity and $\alpha$ enhancement. We generate simulated Hess
diagrams around the main-sequence turn-off region from each set of isochrones
and use a Voronoi binning method to fit the diagrams to HST ACS data. We find
the age of M92 to be $13.80 \pm 0.75$ Gyr. The $5.4\%$ error in the absolute
age is dominated by the uncertainty in the distance to M92 ($\sim 80\%$ of the
error budget); of the remaining parameters, only the total metallicity,
$\alpha$ element abundance, and treatment of helium diffusion contribute
significantly to the total error.
