In this paper we present calculated fractional abundances in dense interstellar clouds for selected atomic and molecular species using three different homogeneous, pseudo-time-dependent models discussed by Bettens, Lee, & Herbst (1995): the new standard model, the new neutral-neutral model, and model 4. We have run each model with 3 different hydrogen densities - 1,000; 10,000; and 100,000cm-3 - and two temperatures - 10K and 50K. "Low metal" elemental abundances have been used for all three models; the new standard model has also been run with "high metal" abundances.