Gradients in the stellar populations of galaxies -e.g., in age, metallicity, IMF -can result in gradients in the stellar mass to light ratio, M * /L. Such gradients imply that the distribution of the stellar mass and light are different. For old stellar populations, such as those typical of early-type galaxies at z ∼ 0, the M * /L gradients are weak if driven by variations in age and metallicity. However, if they are driven by variations in the stellar Initial Mass Function (IMF), then they can be significantly larger. An IMF-driven gradient which has M * /L decreasing outwards from the center increases the estimated total stellar mass (M * ) and reduces the scale which contains half this mass (R e, * ), compared to the values of mass and size when the gradient is ignored. We estimate IMF-gradients from spatially resolved spectra of early-type galaxies in the final release of the MaNGA survey, showing that the fractional decrease in R e, * can be significantly larger than the fractional M * increase, especially when the light is more centrally concentrated. The R e, * −M * correlation which results from the IMF-driven M * /L gradients at z ∼ 0 is offset by almost 0.3 dex to smaller sizes compared to when these gradients are ignored. Comparison with higher redshift samples is not straightforward. If it is fair to compare z ∼ 0 'early-type' galaxies with 'quiescent' galaxies at higher-z, then one must be able to consistently account for evolution in stellar population gradients (especially age and IMF) as well as changes in the steepness of the light profile before drawing conclusions about the evolution of the R e, * − M * relation.