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The Hubble sequence is a common classification scheme for the structure ofgalaxies. Despite the tremendous usefulness of this diagnostic, we still do notfully understand when, where, and how this morphological ordering was put inplace. Here, we investigate the morphological evolution of a sample of 22 highredshift ($z\geq3$) galaxies extracted from the Argo simulation. Argo is acosmological zoom-in simulation of a group-sized halo and its environment. Itadopts the same high resolution ($\sim10^4$ M$_\odot$, $\sim100$ pc) andsub-grid physical model that was used in the Eris simulation but probes asub-volume almost ten times bigger with as many as 45 million gas and starparticles in the zoom-in region. Argo follows the early assembly of galaxieswith a broad range of stellar masses ($\log M_{\star}/{\rm M}_{\odot}\sim8-11$at $z\simeq3$), while resolving properly their structural properties. Werecover a diversity of morphologies, including late-type/irregular discgalaxies with flat rotation curves, spheroid dominated early-type discs, and amassive elliptical galaxy, already established at $z\sim3$. We identify majormergers as the main trigger for the formation of bulges and the steepening ofthe circular velocity curves. Minor mergers and non-axisymmetric perturbations(stellar bars) drive the bulge growth in some cases. The specific angularmomenta of the simulated disc components fairly match the values inferred fromnearby galaxies of similar $M_{\star}$ once the expected redshift evolution ofdisc sizes is accounted for. We conclude that morphological transformations ofhigh redshift galaxies of intermediate mass are likely triggered by processessimilar to those at low redshift and result in an early build-up of the Hubblesequence.

The Argo Simulation: II. The Early Build-up of the Hubble Sequence