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 .