Comparison of the non-spot SPOTS models to those of the MIST collaboration (Choi et al. 2016; Dotter 2016). Left: three isochrones and four evolutionary tracks from SPOTS (red) and MIST (black). Overall the agreement is quite good at early times. Top right: a comparison of the three isochrones from the left panel in the Gaia CMD. The agreement is good at higher masses, but we find substantial departures toward the low-mass end driven by the different calibrations. Middle right: same as top right, except for V versus V − K_S. The agreement is to that seen in the Gaia CMD. Bottom right: same as top right, but in V versus B − V. The agreement is excellent at higher temperatures, but we find very large departures below B − V = 1.3. This results from complications in the MIST color calibrations at the blue end of the spectral energy distribution for low-mass stars.