  A common feature of electromagnetic emission from solar flares is the
presence of intensity pulsations that vary as a function of time. Known as
quasi-periodic pulsations (QPPs), these variations in flux appear to include
periodic components and characteristic time-scales. Here, we analyse a GOES
M3.7 class flare exhibiting pronounced QPPs across a broad band of wavelengths
using imaging and time-series analysis. We identify QPPs in the timeseries of
X-ray, low frequency radio and EUV wavelengths using wavelet analysis, and
localise the region of the flare site from which the QPPs originate via X-ray
and EUV imaging. It was found that the pulsations within the 171 \.A, 1600 \.A,
soft X-ray (SXR), and hard X-ray (HXR) light curves yielded similar periods of
$\sim$122 s, $\sim$131s, $\sim$123 s, and $\sim$137 s, respectively, indicating
a common progenitor. The low frequency radio emission at 2.5 MHz contained a
longer period of $\sim$231 s. Imaging analysis indicates that the location of
the X-ray and EUV pulsations originates from a HXR footpoint linked to a system
of nearby open magnetic field lines. Our results suggest that intermittent
particle acceleration, likely due to 'bursty' magnetic reconnection, is
responsible for the QPPs. The precipitating electrons accelerated towards the
chromosphere produce the X-ray and EUV pulsations, while the escaping electrons
result in low frequency radio pulses in the form of type III radio bursts. The
modulation of the reconnection process, resulting in episodic particle
acceleration, explains the presence of these QPPs across the entire spatial
range of flaring emission.
