  We present the results of the ALMA Large Program Early Planet Formation in
Embedded disks observations of the Class 0 protostar GSS30 IRS3. Our
observations included 1.3 mm continuum with a resolution of 0.''05 (7.8 au) and
several molecular species including $^{12}$CO, $^{13}$CO, C$^{18}$O, H$_{2}$CO
and c-C$_{3}$H$_{2}$. The dust continuum analysis unveiled a disk-shaped
structure with a major axis size of $\sim$200 au. We observed an asymmetry in
the minor axis of the continuum emission suggesting that the emission is
optically thick and the disk is flared. On the other hand, we identified two
prominent bumps along the major axis located at distances of 26 and 50 au from
the central protostar. The origin of the bumps remains uncertain and might be
due to an embedded substructure within the disk or the result of the
temperature distribution instead of surface density due to optically thick
continuum emission. The $^{12}$CO emission reveals a molecular outflow
consisting of three distinct components: a collimated one, an intermediate
velocity component exhibiting an hourglass shape, and a wider angle
low-velocity component. We associate these components with the coexistence of a
jet and a disk-wind. The C$^{18}$O emission traces both a Keplerian rotating
circumstellar disk and the infall of the rotating envelope. We measured a
stellar dynamical mass of 0.35$\pm$0.09 M$_{\odot}$.
