  We investigate the potential of the Atacama Large Millimeter/submillimeter
Array (ALMA) and the Next Generation Very Large Array (ngVLA) to observe
substructures in nearby young disks which are due to the gravitational
interaction between disk material and planets close to the central star. We
simulate the gas and dust dynamics in the disk using the LA-COMPASS
hydrodynamical code. We generate synthetic images for the dust continuum
emission at sub-millimeter to centimeter wavelengths and simulate ALMA and
ngVLA observations. We explore the parameter space of some of the main disk and
planet properties that would produce substructures that can be visible with
ALMA and the ngVLA. We find that ngVLA observations with an angular resolution
of 5 milliarcsec at 3 mm can reveal and characterize gaps and azimuthal
asymmetries in disks hosting planets with masses down to $\approx~5 M_{\oplus}$
$\approx 1 - 5$ au from a Solar-like star in the closest star forming regions,
whereas ALMA can detect gaps down to planetary masses of $\approx
20~M_{\oplus}$ at 5 au. Gaps opened by super-Earth planets with masses $\approx
5 - 10 M_{\oplus}$ are detectable by the ngVLA in the case of disks with low
viscosity ($\alpha \sim 10^{-5}$) and low pressure scale height ($h \approx
0.025$ au at 5 au). The ngVLA can measure the proper motion of azimuthal
asymmetric structures associated with the disk-planet interaction, as well as
possible circumplanetary disks on timescales as short as one to a few weeks for
planets at $1 - 5$ au from the star.
