  We analyze the gamma-ray emission from 9 high latitude, translucent molecular
clouds taken with the Fermi Large Area Telescope (LAT) between 250 MeV and 10
GeV. Observations of gamma-rays allow us to probe the density and spectrum of
cosmic rays in the solar neighborhood. The clouds studied lie within
$\sim\!$270 pc from the Sun and are selected from the Planck all-sky CO map.
Gamma-rays in this energy range mostly result from cosmic ray interactions with
the interstellar medium, which is traced with three components: HI, CO, and
dark gas. Every cloud is detected and shows significant, extended gamma-ray
emission from molecular gas. The gamma-ray emission is dominated by the
CO-emitting gas in some clouds, but by the CO-dark gas in others. The average
emissivity and gamma-ray power law index from HI above 1 GeV shows no evidence
of a systematic variation. The CO-to-H$_2$ conversion factor shows no variation
between clouds over this small spatial range, but shows significant variations
within each cloud. The average CO-to-H$_2$ conversion factor suggests that the
CO-dark gas is molecular as opposed to optically thick HI.
