The combination of high resolution images and large surveys of protoplanetary disks is revealing the general properties of the systems where planets form. On one hand, bright protoplanetary disks show rings and gaps in mm continuum emission that can be easily explained by radial trapping of dust pebbles by embedded planets. However, other mechanisms have been proposed to lead to the same pattern. Recent modelling shows that a key way to distinguish between different scenarios is by looking at spatially resolved molecular line emission. On the other hand, observations are also showing that most protoplanetary disks have very compact emission (< 15 AU), and the properties of these objects is still debated. I will show new ALMA observations of one of these objects at high spatial resolution and sensitivity. These observations indicate that the bulk of the disk population may be very different from the highly structured objects that have been targeted in most campaigns. Finally, I will show new evidence of disk misalignments, which seem to occur for a high fraction of massive disks; this misaligned geometry can deeply affect the final architecture of planets that are born from such natal environments.