Stars form out of the gravitational collapse of centrally condensed cores of dense molecular gas. Systematic observations of molecular emission lines which are excited at the high densities and cold temperatures found in star forming regions have revealed the physical and chemical structure of solar-mass size cores which have formed or may soon form a single star or stellar binary, and form the basis of theories of single-star formation. The initial conditions of star formation in this `isolated' mode have consequently become well-understood. Most stars, however, form in more clustered environments. I will present the results of a systematic effort to determine the initial conditions of clustered, low mass star formation, in the nearby Ophiuchus molecular cloud, through emission maps of molecular species (including NH3, N2H+, N2D+ and H2D+) expected to trace cold, dense gas.