  HIP 67522 b is a 17 Myr old, close-in ($P_{orb} = 6.96$ d), Jupiter-sized ($R
= 10\,R_{\oplus}$) transiting planet orbiting a Sun like star in the Sco-Cen OB
association. We present our measurement of the system's projected orbital
obliquity via two spectroscopic transit observations using the CHIRON
spectroscopic facility. We present a global model that accounts for large
surface brightness features typical of such young stars during spectroscopic
transit observations. With a value of $|\lambda| = 5.8^{+2.8\,\circ}_{-5.7}$,
it is unlikely that this well-aligned system is the result of a high
eccentricity driven migration history. By being the youngest planet with a
known obliquity, HIP 67522 b holds a special place in contributing to our
understanding of giant planet formation and evolution. Our analysis shows the
feasibility of such measurements for young and very active stars.
