  We present the results of Atacama Large Millimeter/Submillimeter Array (ALMA)
108, 233, 352, and 691 GHz continuum observations and Very Large Array (VLA)
4.81 and 8.36 GHz observations of the nearby luminous merger remnant NGC 1614.
By analyzing the beam (1".0 * 1".0) and uv (> 45 k{\lambda}) matched ALMA and
VLA maps, we find that the deconvolved source size of lower frequency emission
(< 108 GHz) is more compact (420 pc * 380 pc) compared to the higher frequency
emission (> 233 GHz) (560 pc * 390 pc), suggesting different physical origins
for the continuum emission. Based on an SED model for a dusty starburst galaxy,
it is found that the SED can be explained by three components, (1) non-thermal
synchrotron emission (traced in the 4.81 and 8.36 GHz continuum), (2) thermal
free-free emission (traced in the 108 GHz continuum), and (3) thermal dust
emission (traced in the 352 and 691 GHz continuum). We also present the
spatially-resolved (sub-kpc scale) Kennicutt-Schmidt relation of NGC 1614. The
result suggests a systematically shorter molecular gas depletion time in NGC
1614 (average {\tau}_gas of 49 - 77 Myr and 70 - 226 Myr at the starburst ring
and the outer region, respectively) than that of normal disk galaxies (~ 2 Gyr)
and a mid-stage merger VV 114 (= 0.1 - 1 Gyr). This implies that the star
formation activities in U/LIRGs are efficiently enhanced as the merger stage
proceeds, which is consistent with the results from high-resolution numerical
merger simulations.
