  New 3.3--3.6~$\mu$m spectra were obtained of nine young stellar objects
embedded in molecular clouds. An absorption feature at $\sim$3.47~$\mu$m
(2880~cm$^{-1}$) with FWHM$\sim$0.09 $\mu$m (80 cm$^{-1}$), first identified by
Allamandola et al. (1992), was definitively detected toward seven objects, and
marginally in the other two. The feature is better correlated with H$_2$O ice
than with the silicate dust optical depth in the data obtained to date.
Assuming the feature is due to a C--H stretch absorption, the abundance of the
C--H bonds averaged along the lines of sight is closely related to that of
H$_2$O ice. We interpret the correlation with H$_2$O ice as indicating that the
C--H bonds form together with H$_2$O ice on grain surfaces in the molecular
clouds, though other formation mechanisms are not ruled out. A second
absorption feature at 3.25 $\mu$m (3080 cm$^{-1}$) was detected toward
NGC7538/IRS 1 and S140/IRS 1; this feature was first detected in spectra of
MonR2/IRS 3 (Sellgren, Smith, \& Brooke 1994; Sellgren et al. 1995). There is
as yet insufficient data to tell whether this feature is better correlated with
H$_2$O ice or silicates.
