Color difference between the rotating and nonrotating MS stellar models with an LMC metallicity as a function of absolute magnitude M_F814W, 0 at four different ages, which are the zero-age and the derived ages for three young LMC clusters NGC 1755 (80 Myr), NGC 2164 (100 Myr) and NGC 1866 (200 Myr) (Milone et al. 2018). The solid, dashed, and dotted lines denote our MESA models, the SYCLIST models and the MIST models, respectively, color-coded by their initial rotational rates. The formally labeled fractional critical angular velocities of the SYCLIST models in their web interface are shown in parentheses. Shaded areas show the Δcolor range occupied by stars with orientations that are between pole-on and equator-on. The dots with error bars in the last three panels indicate the color difference between the red and blue MSs of the abovementioned three clusters (see Fig. 5 in Milone et al. 2016 for NGC 1755, Fig. 13 in Milone et al. 2018 for NGC 2164 and Fig. 6 in Milone et al. 2017 for NGC 1866, respectively). We only consider the unevolved stars below the cluster turnoff (see text). The error bars on the x-axis mean photometric errors while the error bars on the y-axis correspond to magnitude intervals.