  Magnetic fields likely play an important role in star formation, but the
number of directly measured magnetic field strengths remains scarce. We
observed the 38.3 and 38.5 GHz Class II methanol (CH$_3$OH) maser lines toward
the high mass star forming region NGC 6334F for the Zeeman effect. The observed
spectral profiles have two prominent velocity features which can be further
decomposed through Gaussian component fitting. In several of these fitted
Gaussian components we find significant Zeeman detections, with $zB_{\rm los}$
in the range from 8 to 46 Hz. If the Zeeman splitting factor $z$ for the 38 GHz
transitions is of the order of $\sim$1 Hz mG$^{-1}$, similar to that for
several other CH$_3$OH maser lines, then magnetic fields in the regions traced
by these masers would be in the range of 8-46 mG. Such magnetic field values in
high mass star forming regions agree with those detected in the better-known
6.7 GHz Class II CH$_3$OH maser line. Since Class II CH$_3$OH masers are
radiatively pumped close to the protostar and likely occur in the accretion
disk or the interface between the disk and outflow regions, such fields likely
have significant impact on the dynamics of these disks.
