  We have conducted mapping observations toward the n3 and n5 positions in the
NGC\,2264-D cluster-forming region with the Atacama Compact Array (ACA) of the
Atacama Large Millimeter/submillimeter Array (ALMA) in Band 3. Observations
with 10000 au scale beam reveal the chemical composition at the clump scale.
The spatial distributions of the observed low upper-state-energy lines of
CH$_{3}$OH are similar to those of CS and SO, and the HC$_{3}$N emission seems
to be predominantly associated with clumps containing young stellar objects.
The turbulent gas induced by the star formation activities produces large-scale
shock regions in NGC\,2264-D, which are traced by the CH$_{3}$OH, CS and SO
emissions. We derive the HC$_{3}$N, CH$_{3}$CN, and CH$_{3}$CHO abundances with
respect to CH$_{3}$OH. Compared to the n5 field, the n3 field is farther (in
projected apparent distance) from the neighboring NGC\,2264-C, yet the chemical
composition in the n3 field tends to be similar to that of the protostellar
candidate CMM3 in NGC\,2264-C. The HC$_{3}$N/CH$_{3}$OH ratios in the n3 field
are higher than those in the n5 field. We find an anti-correlation between the
HC$_{3}$N/CH$_{3}$OH ratio and their excitation temperatures. The low
HC$_{3}$N/CH$_{3}$OH abundance ratio at the n5 field implies that the n5 field
is an environment with more active star formation compared with the n3 field.
