  Investigating the physical and chemical structures of massive star-forming
regions is critical for understanding the formation and the early evolution of
massive stars. We performed a detailed line survey toward six dense cores named
as MM1, MM4, MM6, MM7, MM8, and MM11 in G9.62+0.19 star-forming region resolved
in ALMA band 3 observations. Toward these cores, about 172 transitions have
been identified and attributed to 16 species including organic Oxygen-,
Nitrogen-, Sulfur-bearing molecules and their isotopologues. Four dense cores
MM7, MM8, MM4, and MM11 are line rich sources. Modeling of these spectral lines
reveals the rotational temperature in a range of 72$-$115~K, 100$-$163~K,
102$-$204~K, and 84$-$123~K for the MM7, MM8, MM4, and MM11, respectively. The
molecular column densities are 1.6 $\times$ 10$^{15}$ $-$ 9.2 $\times$
10$^{17}$~cm$^{-2}$ toward the four cores. The cores MM8 and MM4 show chemical
difference between Oxygen- and Nitrogen-bearing species, i.e., MM4 is rich in
oxygen-bearing molecules while nitrogen-bearing molecules especially
vibrationally excited HC$_{3}$N lines are mainly observed in MM8. The distinct
initial temperature at accretion phase may lead to this N/O differentiation.
Through analyzing column densities and spatial distributions of O-bearing
Complex Organic Molecules (COMs), we found that C$_{2}$H$_{5}$OH and
CH$_{3}$OCH$_{3}$ might have a common precursor, CH$_{3}$OH. CH$_{3}$OCHO and
CH$_{3}$OCH$_{3}$ are likely chemically linked. In addition, the observed
variation in HC$_{3}$N and HC$_{5}$N emission may indicate that their different
formation mechanism at hot and cold regions.
