  High-resolution imaging of galaxies in rest-frame UV has revealed the
existence of giant star-forming clumps prevalent in high redshift galaxies.
Studying these sub-structures provides important information about their
formation and evolution and informs theoretical galaxy evolution models. We
present a new method to identify clumps in galaxies' high-resolution rest-frame
UV images. Using imaging data from CANDELS and UVCANDELS, we identify
star-forming clumps in an HST/F160W$\leq 25$ AB mag sample of 6767 galaxies at
$0.5\leq z\leq 3$ in four fields, GOODS-N, GOODS-S, EGS, and COSMOS. We use a
low-pass band filter in Fourier space to reconstruct the background image of a
galaxy and detect small-scale features (clumps) on the background-subtracted
image. Clumpy galaxies are defined as those having at least one off-center
clump that contributes a minimum of 10$\%$ of the galaxy's total rest-frame UV
flux. We measure the fraction of clumpy galaxies ($\rm f_{clumpy}$) as a
function of stellar mass, redshift, and galaxy environment. Our results
indicate that $\rm f_{clumpy}$ increases with redshift, reaching $\sim 65\%$ at
$z\sim 1.5$. We also find that $\rm f_{clumpy}$ in low-mass galaxies ($\rm
9.5\leq log(M_*/M_\odot)\leq 10$) is 10$\%$ higher compared to that of their
high-mass counterparts ($\rm log(M_*/M_\odot)>10.5$). Moreover, we find no
evidence of significant environmental dependence of $\rm f_{clumpy}$ for
galaxies at the redshift range of this study. Our results suggest that the
fragmentation of gas clouds under violent disk instability remains the primary
driving mechanism for clump formation, and incidents common in dense
environments, such as mergers, are not the dominant processes.
