We have carried out interferometric observations of cyanopolyynes, HC\(_{3}\)N, HC\(_{5}\)N, and HC\(_{7}\)N, in the 36 GHz band toward the G28.28\(-\)0.36 high-mass star-forming region using the Karl G. Jansky Very Large Array (VLA) Ka-band receiver. The spatial distributions of HC\(_{3}\)N and HC\(_{5}\)N are obtained. HC\(_{5}\)N emission is coincident with a 450 \(\mu\)m dust continuum emission and this clump with a diameter of \(\sim 0.2\) pc is located at the east position from the 6.7 GHz methanol maser by \(\sim 0.15\) pc. HC\(_{7}\)N is tentatively detected toward the clump. The HC\(_{3}\)N : HC\(_{5}\)N : HC\(_{7}\)N column density ratios are estimated at 1.0 : \(\sim 0.3\) : \(\sim 0.2\) at an HC\(_{7}\)N peak position. We discuss possible natures of the 450 \(\mu\)m continuum clump associated with the cyanopolyynes. The 450 \(\mu\)m continuum clump seems to contain deeply embedded low- or intermediate-mass protostellar cores, and the most possible formation mechanism of the cyanopolyynes is the warm carbon chain chemistry (WCCC) mechanism. In addition, HC\(_{3}\)N and compact HC\(_{5}\)N emission is detected at the edge of the 4.5 \(\mu\)m emission, which possibly implies that such emission is the shock origin.