  We present new observations of [CII] fine structure line emission from an
isolated molecular cloud using the upGREAT instrument onboard SOFIA. These data
are analyzed together with archival CO=1-0 and HI 21 cm emission spectra to
investigate the role of converging atomic gas flows in the formation of
molecular clouds. Bright [CII] emission is detected throughout the mapped area
that likely originates from photodissociation regions excited by UV radiation
fields produced by newborn stars within the cloud. Upon spatial averaging of
the [CII] spectra, we identify weak [CII] emission within velocity intervals
where the HI 21 cm line is brightest; these are blue-shifted relative to
velocities of the CO and bright [CII] emission by 4 km/s. The brightness
temperatures, velocity dispersions, and alignment with HI 21 cm velocities
connect this [CII] emission component to the cold, neutral atomic gas of the
interstellar medium (CNM). We propose that this CNM feature is an accretion
flow onto the far--side of the existing molecular cloud. The mass infall rate
is 3.2x10**{-4} Msun/yr. There is no direct evidence of a comparable
red--shifted component in the [CII] or HI 21 cm spectral lines that would
indicate the presence of a converging flow.
