  Mapping the orbital obliquity distribution of young planets is one avenue
towards understanding mechanisms that sculpt the architectures of planetary
systems. TOI-942 is a young field star, with an age of ~60 Myr, hosting a
planetary system consisting of two transiting Neptune-sized planets in 4.3- and
10.1-day period orbits. We observed the spectroscopic transits of the inner
Neptune TOI-942b to determine its projected orbital obliquity angle. Through
two partial transits, we find the planet to be in a prograde orbit, with a
projected obliquity angle of |lambda| = 1/+41-33 deg. In addition,
incorporating the light curve and the stellar rotation period, we find the true
three-dimensional obliquity to be 2/+27-23 deg. We explored various sources of
uncertainties specific to the spectroscopic transits of planets around young
active stars, and showed that our reported obliquity uncertainty fully
encompassed these effects. TOI-942b is one of the youngest planets to have its
obliquity characterized, and one of even fewer residing in a multi-planet
system. The prograde orbital geometry of TOI-942b is in line with systems of
similar ages, none of which have yet been identified to be in strongly
misaligned orbits.
