  The Gaia mission has provided highly accurate observations that have
significantly reduced the scatter in the colour-magnitude diagrams of open
clusters. As a result of the improved isochrone sequence of the open cluster
M67, we have created new stellar models that avoid commonly used
simplifications in 1D stellar modelling, such as mass-independent core
overshooting and a constant mixing length parameter. This has enabled us to
deliver a precise isochrone specifically designed for M67, available for
download. We follow a commonly used qualitative approach to adjust the input
physics to match the well-defined colour-magnitude sequence, and we test the
model-predicted masses against a known eclipsing binary system at the main
sequence turnoff of the cluster. Despite using improvements in photometry and
stellar physics we cannot match the masses of both binary components with the
same theoretical isochrone. A chi-square-based isochrone fitting approach using
our preferred input physics results in a cluster age of 3.95+0.16-0.15 Gyrs.
