Chemical data for 31 major, minor, and trace elements were obtained by instrumental neutron activation analysis (INAA) for bulk and size fractions of drive tubes 14210/11 (39 cm) and 14220 (16.5 cm) and soils 14141, 14148, and 14149. Both cores are KREEPy and homogeneous in chemical composition. The meteoritic component varies from 3 to 7% in both cores. The heterogeneous Ni profiles suggest little in situ mixing of the cores since their emplacements. The bulk soils on the average contain 20% low-K-Fra Mauro basalt (LKFM) (62295), 10 to 15% mare basalt (14072), 6% anorthosite-norite-troctolite (ANT) and 59% high-K KREEP. There are no significant intrasite chemical variations at the Apollo 14 site. Among the grain sizes, the coarse 1000-90, 90--20, and 20--10 μm fractions are similar in chemistry, but quite different from the <10 μm fine fractions. The <10 μm fine fractions comprise 5 to 15% of the bulk soils and are consistently more feldspathic and enriched in incompatible (LIL) elements relative to the coarse fractions. In the mature soils, agglutinates dominate the chemistry of the coarser fractions, and the similarity of LIL contents between the 1000-90 μm fractions and the <10 μm fine fractions strongly suggests that agglutinates are derived from the fine fraction, which supports the F3 model of Papike et al. <1981>. Relative to the bulk soil, the <10 μm fine fraction is enriched in Al2O3, CaO, Na2O, K2O, Ba, Sr, La (REE), Eu, and Th and depleted in MgO, FeO, Mn, and Sc. The observed varying degrees of enrichments and depletions can largely be explained by simple comminution of mesostasis and feldspar and their preferential incorporation into the finest fraction. Lateral mixing over short distances, simple comminution, and veritical mixing of the regolith are the dominant soil-forming processes.