We present near-infrared imaging spectroscopy of the strongly-lensed z = 2.00 galaxy SDSS J120601.69+514227.8 ( ‘ the Clone arc ’ ) . Using OSIRIS on the Keck 2 telescope with laser guide star adaptive optics , we achieve resolved spectroscopy with 0.20 arcsecond FWHM resolution in the diagnostic emission lines [ O iii ] , H \alpha , and [ N ii ] . The lensing magnification allows us to map the velocity and star formation from H \alpha emission at a physical resolution of \simeq 300 pc in the galaxy source plane . With an integrated star formation rate of \simeq 50 M _ { \odot } yr ^ { -1 } , the galaxy is typical of sources similarly studied at this epoch . It is dispersion-dominated with a velocity gradient of \simeq \pm 80 km s ^ { -1 } and average dispersion \bar { \sigma } = 85 km s ^ { -1 } ; the dynamical mass is 2.4 \times 10 ^ { 10 } M _ { \odot } within a half-light radius of 2.9 kpc . Robust detection of [ N ii ] emission across the entire OSIRIS field of view enables us to trace the gas-phase metallicity distribution with 500 pc resolution . We find a strong radial gradient in both the [ N ii ] /H \alpha and [ O iii ] /H \alpha ratios indicating a metallicity gradient of -0.27 \pm 0.05 dex kpc ^ { -1 } with central metallicity close to solar . We demonstrate that the gradient is seen independently in two multiple images . While the physical gradient is considerably steeper than that observed in local galaxies , in terms of the effective radius at that epoch , the gradient is similar . This suggests that subsequent growth occurs in an inside-out manner with the inner metallicity gradient diminished over time due to radial mixing and enrichment from star formation .