  We use extensive global two-dimensional hydrodynamic disk gas+dust
simulations with embedded planets, coupled with three dimensional radiative
transfer calculations, to model the dust ring and gap structures in the HL Tau
protoplanetary disk observed with the Atacama Large Millimeter/Submillimeter
Array (ALMA). We include the self-gravity of disk gas and dust components and
make reasonable choices of disk parameters, assuming an already settled dust
distribution and no planet migration. We can obtain quite adequate fits to the
observed dust emission using three planets with masses 0.35, 0.17, and 0.26
$M_{Jup}$ at 13.1, 33.0, and 68.6 AU, respectively. Implications for the planet
formation as well as the limitations of this scenario are discussed.
