Abstract We use CEERS JWST/NIRCam imaging to measure rest-frame near-IR light profiles of 435 M _⋆ > 10¹⁰ M _⊙ galaxies in the redshift range of 0.5 < z < 2.3. We compare the resulting rest-frame 1.5–2 μm half-light radii (R _NIR) with stellar half-mass radii ( R M ⋆ ) derived with multicolor light profiles from CANDELS Hubble Space Telescope imaging. In general agreement with previous work, we find that R _NIR and R M ⋆ are up to 40% smaller than the rest-frame optical half-light radius R _opt. The agreement between R _NIR and R M ⋆ is excellent, with a negligible systematic offset (<0.03 dex) up to z = 2 for quiescent galaxies and up to z = 1.5 for star-forming galaxies. We also deproject the profiles to estimate R M ⋆ , 3 D , the radius of a sphere containing 50% of the stellar mass. We present the R−M _⋆ distribution of galaxies at 0.5 < z < 1.5, comparing R _opt, R M ⋆ , and R M ⋆ , 3 D . The slope is significantly flatter for R M ⋆ and R M ⋆ , 3 D compared to R _opt, mostly due to downward shifts in size for massive star-forming galaxies, while R M ⋆ and R M ⋆ , 3 D do not show markedly different trends. Finally, we show rapid evolution of the size (R ∝ (1 + z)^−1.7±0.1) of massive (M _⋆ > 10¹¹ M _⊙) quiescent galaxies between z = 0.5 and z = 2.3, again comparing R _opt, R M ⋆ , and R M ⋆ , 3 D . We conclude that the main tenets of the evolution of the size narrative established over the past 20 yr, based on rest-frame optical light profile analysis, still hold in the era of JWST/NIRCam observations in the rest-frame near-IR.