  Recent ALMA observations on disk substructures suggest the presence of
embedded protoplanets in a large number disks. The primordial configurations of
these planetary systems can be deduced from the morphology of the disk
substructure and serve as initial conditions for numerical investigation of
their future evolution. Starting from the initial configurations of 12
multi-planetary systems deduced from ALMA disks, we carried out two-stage
N-body simulation to investigate the evolution of the planetary systems at the
disk stage as well as the long term orbital stability after the disk dispersal.
At the disk stage, our simulation includes both the orbital migration and
pebble/gas accretion effects. We found a variety of planetary systems are
produced and can be categorised into distant giant planets, Jupiter-like
planets, Neptune-like planets and distant small planets. We found the disk
stage evolution as well as the final configurations are sensitive to both the
initial mass assignments and viscosity. After the disk stage, we implement only
mutual gravity between star and planets and introduce stochastic perturbative
forces. All systems are integrated for up to 10 Gyr to test their orbital
stability. Most planetary systems are found to be stable for at least 10 Gyr
with perturbative force in a reasonable range. Our result implies that a strong
perturbation source such as stellar flybys is required to drive the planetary
system unstable. We discuss the implications of our results on both the disk
and planet observation, which may be confirmed by the next generation
telescopes such as JWST and ngVLA.
