  We present simulations of the capabilities of the Atacama Large
Millimeter/submillimeter Array (ALMA) and of a Next Generation Very Large Array
(ngVLA) to detect and resolve substructures due to terrestrial planets and
Super-Earths in nearby planet-forming disks. We adopt the results of global 2-D
hydrodynamical planet-disk simulations that account for the dynamics of gas and
dust in a disk with an embedded planet. Our simulations follow the combined
evolution of gas and dust for several thousand planetary orbits. We show that
long integrations (several tens of hours) with the ngVLA can detect and
spatially resolve dust structures due to low-mass rocky planets in the
terrestrial planet formation regions of nearby disks (stellocentric radii $r =
1 - 3$ au), under the assumption that the disk viscosity in those regions is
low ($\alpha \le 10^{-5}$). ALMA is instead unable to resolve these structures
in these disk regions. We also show that high-resolution ngVLA observations
separated by several days to few weeks would allow to detect the proper motion
of the azimuthally asymmetric structures expected in the disk regions of
terrestrial planet formation.
