  The spin-orbit obliquity of a planetary system constraints its formation
history. A large obliquity may either indicate a primordial misalignment
between the star and its gaseous disk or reflect the effect of different
mechanisms tilting planetary systems after formation. Observations and
statistical analysis suggest that system of planets with sizes between 1 and 4
R$_{\oplus}$ have a wide range of obliquities ($\sim0-30^{\circ}$), and that
single- and multi-planet transiting have statistically indistinguishable
obliquity distributions. Here, we revisit the ``breaking the chains'' formation
model with focus in understanding the origin of spin-orbit obliquities. This
model suggests that super-Earths and mini-Neptunes migrate close to their host
stars via planet-disk gravitational interactions, forming chain of planets
locked in mean-motion resonances. After gas-disk dispersal, about 90-99\% of
these planetary systems experience dynamical instabilities, which spread the
systems out. Using synthetic transit observations, we show that if planets are
born in disks where the disk angular momentum is virtually aligned with the
star's rotation spin, their final obliquity distributions peak at about $\sim$5
degrees or less, and the obliquity distributions of single and multi-planet
transiting systems are statistically distinct. By treating the star-disk
alignment as a free-parameter, we show that the obliquity distributions of
single and multi-planet transiting systems only become statistically
indistinguishable if planets are assumed to form in primordially misaligned
natal disks with a ``tilt'' distribution peaking at $\gtrsim$10-20 deg. We
discuss the origin of these misalignments in the context of star formation and
potential implications of this scenario for formation models.
