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We report on the gas-phase metallicity gradients of a sample of 264star-forming galaxies at 0.6 < z < 2.6, measured through deep near-infraredHubble Space Telescope slitless spectroscopy. The observations include 12-orbitdepth Hubble/WFC3 G102 grism spectra taken as a part of the CANDELS LyaEmission at Reionization (CLEAR) survey, and archival WFC3 G102+G141 grismspectra overlapping the CLEAR footprint. The majority of galaxies (84%) in thissample are consistent with a zero or slightly positive metallicity gradientacross the full mass range probed (8.5 < log M_*/M_sun < 10.5). We measure theintrinsic population scatter of the metallicity gradients, and show that itincreases with decreasing stellar mass---consistent with previous reports inthe literature, but confirmed here with a much larger sample. To understand thephysical mechanisms governing this scatter, we search for correlations betweenthe observed gradient and various stellar population properties at fixed mass.However, we find no evidence for a correlation with the galaxy properties weconsider---including star-formation rates, sizes, star-formation rate surfacedensities, and star-formation rates per gravitational potential energy. We usethe observed weakness of these correlations to provide material constraints forpredicted intrinsic correlations from theoretical models.

CLEAR: The Gas-Phase Metallicity Gradients of Star-Forming Galaxies at 0.6 < z < 2.6