  Giant star-forming clumps are a prominent feature of star-forming galaxies
(SFGs) and contain important clues on galaxy formation and evolution. However,
basic demographics of clumps and their host galaxies remain uncertain. Using
the HST/WFC3 F275W images from the Ultraviolet Imaging of the Cosmic Assembly
Near-infrared Deep Extragalactic Legacy Survey (UVCANDELS), we detect and
analyze giant star-forming clumps in galaxies at 0.5 $\leq$ z $\leq$ 1,
connecting two epochs when clumps are common (at cosmic high-noon, z $\sim$ 2)
and rare (in the local universe). We construct a clump sample whose rest-frame
1600 {\AA} luminosity is 3 times higher than the most luminous local HII
regions (M$_{UV} \leq -$16 AB). In our sample, 35 $\pm$ 3$\%$ of low-mass
galaxies (log[M$_{*}$/M$_{\odot}$] $<$ 10) are clumpy (i.e., containing at
least one off-center clump). This fraction changes to 22 $\pm$ 3$\%$ and 22
$\pm$ 4$\%$ for intermediate (10 $\leq$ log[M$_{*}$/M$_{\odot}$] $\leq$ 10.5)
and high-mass (log[M$_{*}$/M$_{\odot}$] $>$ 10.5) galaxies in agreement with
previous studies. When compared to similar-mass non-clumpy SFGs, low- and
intermediate-mass clumpy SFGs tend to have higher SFRs and bluer rest-frame U-V
colors, while high-mass clumpy SFGs tend to be larger than non-clumpy SFGs.
However, clumpy and non-clumpy SFGs have similar S\'ersic index, indicating a
similar underlying density profile. Furthermore, we investigate how UV
luminosity of star-forming regions correlates with the physical properties of
host galaxies. On average, more luminous star-forming regions reside in more
luminous, smaller, and/or higher-specific SFR galaxies and are found closer to
their hosts' galactic center.
