Protoplanetary disks are where planets are formed at an uncertain, unknown point; in the last years, the efforts to understand planet formation have focused mainly on Class II protostars. The ALMA Large Program Early Planet Formation in Embedded disks aims to study the origin of substructures in Class 0/I protoplanetary disks with Band 6 at high resolution. Here, we present the results of GSS30 IRS3 with a resolution of 8 au. We detected two bumps in the dust disk modeled using frank, showing that they may be the precursor of more evolved substructures. The C18O gaseous fits a keplerian disk with SLAM and EDDY, fitting a dynamical mass of 0.22 Msun. The C18O also shows a spiral shape close to the systemic velocity that we link with an asymmetric infall; this was proved in the residuals of the EDDY fitting as a red stream. Furthermore, the system has a low-velocity molecular outflow and a high-velocity jet based on the 12CO emission line, which was possible to distinguish due to the high spatial resolution. Finally, the dust disk has enough material to form rocky planets and Jupiter mass planets.