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Current generation stellar isochrone models exhibit non-negligiblediscrepancies due to variations in the input physics. The success of each modelis determined by how well it fits the observations, and this paper aims todisentangle contributions from the various physical inputs. New deep,wide-field optical and near-infrared photometry ($UBVRIJHK_S$) of the clusterM35 is presented, against which several isochrone systems are compared: Padova,PARSEC, Dartmouth and Y$^2$. Two different atmosphere models are applied toeach isochrone: ATLAS9 and BT-Settl. For any isochrone set and atmospheremodel, observed data are accurately reproduced for all stars more massive then$0.7$ M$_\odot$. For stars less massive than 0.7 M$_\odot$, Padova and PARSECisochrones consistently produce higher temperatures than observed. Dartmouthand Y$^2$ isochrones with BT-Settl atmospheres reproduce optical dataaccurately, however they appear too blue in IR colors. It is speculated thatmolecular contributions to stellar spectra in the near-infrared may not befully explored, and that future study may reconcile these differences.

WIYN Open Cluster Study LXII: Comparison of Isochrone Systems using Deep Multi-Band Photometry of M35