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Studying giant star-forming clumps in distant galaxies is important tounderstand galaxy formation and evolution. At present, however, observers andtheorists have not reached a consensus on whether the observed "clumps" indistant galaxies are the same phenomenon that is seen in simulations. In thispaper, as a step to establish a benchmark of direct comparisons betweenobservations and theories, we publish a sample of clumps constructed torepresent the commonly observed "clumps" in the literature. This samplecontains 3193 clumps detected from 1270 galaxies at $0.5 \leq z < 3.0$. Theclumps are detected from rest-frame UV images, as described in our previouspaper. Their physical properties, e.g., rest-frame color, stellar mass (M*),star formation rate (SFR), age, and dust extinction, are measured by fittingthe spectral energy distribution (SED) to synthetic stellar population models.We carefully test the procedures of measuring clump properties, especially themethod of subtracting background fluxes from the diffuse component of galaxies.With our fiducial background subtraction, we find a radial clump U-V colorvariation, where clumps close to galactic centers are redder than those inoutskirts. The slope of the color gradient (clump color as a function of theirgalactocentric distance scaled by the semi-major axis of galaxies) changes withredshift and M* of the host galaxies: at a fixed M*, the slope becomes steepertoward low redshift, and at a fixed redshift, it becomes slightly steeper withM*. Based on our SED-fitting, this observed color gradient can be explained bya combination of a negative age gradient, a negative E(B-V) gradient, and apositive specific star formation rate gradient of the clumps. We also find thatthe color gradients of clumps are steeper than those of intra-clump regions.[Abridged]

Clumpy Galaxies in CANDELS. II. Physical Properties of UV-bright Clumps at $0.5\leq z<3$